Jun 2, 2008 - Life: Disks from birth to maturity, Survey of. KBOs, Planets around nearby stars. NIRCam and its coronagraph image and characterize disks and ...
Building for the James Webb Space Telescope: The Near-Infrared Camera
Marcia Rieke Steward Observatory 02 June 2008 American Astronomical Society, St. Louis, MO
With help from the NIRCam Team:
Scott Horner2, Doug Kelly1, John Stansberry1, Erick Young1, Daniel Eisenstein1, Don McCarthy1, Michael Meyer1, George Rieke1, Chad Engelbracht1, Stefi Baum3, Chas Beichman4, John Krist4, René Doyon5, Alan Dressler6, Laura Ferrarese7, Tom Greene8, Don Hall9, Klaus Hodapp9, Doug Johnstone7, Simon Lilly10,Peter Martin11, Tom Roellig8, John Stauffer12, John Trauger4 1Steward Observatory, University of Arizona; 2Lockheed Martin Advanced Technology Center, 3RIT, 4JPL, 5U.Montreal, 6Carnegie Obs., 7HIA/DAO, 8 NASA/ARC, 9U. Hawaii, 10ETH Zurich, 11U. Toronto, 12Spitzer Science Center
A PI’s Motivation
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A Journey Begun in ~1998 JWST has been contemplated for quite awhile -- started with “HST and Beyond” which recommended a 4-m Dan Goldin upped the ante to an 8-meter – reality forced a reduction back to 6.5-meter
3
What’s NIRCam?
• NIRCam is the near-infrared camera (0.6-5 microns) for JWST
Optical Telescope Element (OTE)
1m
Integrated Science Instrument Module (ISIM)
Primary Mirror
• NIRCam is the wavefront sensor
Cold, spacefacing side
Spacecraft Bus Sunshield
¾ Refractive design to minimize mass and volume ¾ Dichroic used to split range into short (0.6-2.3μm) and long (2.45μm) sections ¾ Nyquist sampling at 2 and 4μm ¾ 2.2 arc min x 4.4 arc min total field of view seen in two colors (40 MPixels) ¾ Coronagraphic capability for both short and long wavelengths
Warm, Sun-facing Sun-facing side side Warm,
¾ Must be fully redundant ¾ Dual filter/pupil wheels to accommodate WFS hardware ¾ Pupil imaging lens to check optical alignment 4
JWST Overview • 25 m2 collecting area using a segmented primary with 6.6-m tip-to-tip diameter: Resolution at 2μm = 0.06 arc sec • L2 orbit enables passive cooling to ~45K for primary mirror, ~35K for instruments • Four instruments: ¾NIRCam, 0.6-5 µm ¾NIRSpec, 0.6-5 µm, R~100-3000 and multi-object ¾FGS + TF, 1.8-4.8 µm R~100 ¾MIRI, 5-28 µm, camera + R~2500 IFUs
• To be launched in 2013 on an Ariane V
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Project is moving! • •
Primary mirror segments and detectors are already in production Instruments are building verification and engineering test units NIRCam qualification focal plane. NIRCam ETU bench. MIRI Verification model prior to testing. today 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 Concept Development
science operations
Design, Fabrication, Assembly and Test
NIRCam delivery mission formulation authorized
confirmation for mission implementation
launch
www.JWST.nasa.gov 6
Mirror Fabrication Raw Be billet (two mirrors)
JWST mirrors made of beryllium Lightweight and stable at 40 K Primary mirror segment Secondary mirror Tertiary mirror
Machined, lightweighted mirrors 95% of material is removed
Polished mirrors Mirror segment figure ~ 20 nm Courtesy of M. Clampin 7
Mirror Polishing on Schedule JWST has all 18 flight mirrors undergoing polishing at Tinsley Pathfinder C7 22%
LEGEND Not at L-3 SSG-Tinsley
EDU
Flight
EDU-B 75%
SM1 29%
C6 42% B8 23%
Even Slice Figure Grind Smooth Out Grind Rough Polish
C5 51%
Smooth Out Polish Fine Figure Polish Shipped to Cryo Cryo Null Figure Final Optical Test Delivered – – – – – Pathfinder
B7 42%
A6 43% A5 54%
B2 55% A1 64% SM2 4% A4 56%
C4 51% B6 53%
Flight TM1 15%
C1 53% A2 57%
B3 59%
FSM 90%
C2 57%
A3 51% C3 59%
B5 54% As of 05/17/08
Courtesy of M. Clampin 8
NIRCam NIRCAM_X000
Modern Universe
Clusters & Morphology
Reionoization
First Galaxies
Recombination
Forming Atomic Nuclei
Inflation
Quark Soup
NIRCam’s Role in JWST’s Science Themes The First Light in the Universe: Discovering the first galaxies, Reionization NIRCam executes deep surveys to find and categorize objects.
Period of Galaxy Assembly: Establishing the Hubble sequence, Growth of galaxy clusters NIRCam provides details on shapes and colors of galaxies, identifies young clusters
Stars and Stellar Systems: Physics of the IMF,
young solar system Kuiper Belt
Planets
Structure of pre-stellar cores, Emerging from the dust cocoon NIRCam measures colors and numbers of stars in clusters, measure extinction profiles in dense clouds
Planetary Systems and the Conditions for Life: Disks from birth to maturity, Survey of KBOs, Planets around nearby stars NIRCam and its coronagraph image and characterize disks and planets, classifies surface properties of KBOs 9
NIRCam Science Requirements (1) •
Detection of first light objects requires: ¾ Highest possible sensitivity – few nJy sensitivity is required. ¾ Fields of view (~10 square arc minute) adequate for detecting rare first light sources in deep multi-color surveys. ¾ A filter set capable of yielding ~4% rms photometric redshifts for >98% of the galaxies in a deep multi-color survey.
•
Observing the period of galaxy assembly requires in addition to above: high spatial resolution for distinguishing shapes of galaxies at the sub-kpc scale (at the diffraction limit of a 6.5m telescope at 2µm). Performance of adopted filter set 4 Number of Filters
1000
6
100
4 Number of Filters
5-σ 50,000 secs 10
5 6 7
1
4 Number of Filters
nJy
5
0.1 0.5
1.5
2.5
3.5
4.5
Space (HST or SPITZER)
6 7 8
l(m m) Ground (Keck/VLT)
5
0.00
NIRCam
z=5.0
z=10.1
1
